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Siebert, A; Famaey, B; Binney, J; Burnett, B; Faure, C; Minchev, I; Williams, M. E. K; Bienaymé, O; Bland-Hawthorn, J; Boeche, C; Gibson, B. K; Grebel, E. K; Helmi, A; Just, A; Munari, U; Navarro, J. F; Parker, Q. A; Reid, W. A; Seabroke, G; Siviero, A; Steinmetz, M; Zwitter, T
Monthly notices of the Royal Astronomical Society, 21 September 2012, Letnik: 425, Številka: 3Journal Article
Abstract Using the Radial Velocity Experiment (RAVE) survey, we recently brought to light a gradient in the mean galactocentric radial velocity of stars in the extended solar neighbourhood. This gradient likely originates from non-axisymmetric perturbations of the potential, among which a perturbation by spiral arms is a possible explanation. Here, we apply the traditional density wave theory and analytically model the radial component of the two-dimensional velocity field. Provided that the radial velocity gradient is caused by relatively long-lived spiral arms that can affect stars substantially above the plane, this analytic model provides new independent estimates for the parameters of the Milky Way spiral structure. Our analysis favours a two-armed perturbation with the Sun close to the inner ultra-harmonic 4:1 resonance, with a pattern speed and a small amplitude per cent of the background potential (14 per cent of the background density). This model can serve as a basis for numerical simulations in three dimensions, additionally including a possible influence of the Galactic bar and/or other non-axisymmetric modes.
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JCR | SNIP | JCR | SNIP | JCR | SNIP | JCR | SNIP |
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in: SICRIS
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